Chandra X-Ray Observatory
	(CXC)

Accepted Cycle 9 Observing Proposals

CLUSTERS OF GALAXIES

Proposal Number Type PI Name Title
09800046 GTO/TOO Gordon Garmire Chandra Observations of SZ-selected Galaxy Clusters Detected by the South Pole Telescope
09800120 GTO/TOO Stephen Murray South Pole Telescope (SPT) - Chandra Cluster Cosmology
09800154 GO Stefano Andreon Characterisation of the most distant cluster of galaxies, JKCS041 at z=1.91
09800310 LP Steven Allen Probing Dark Energy with Relaxed Galaxy Clusters
09800313 GO Steven Allen Bubble heating in Extreme Cooling Clusters
09800349 GO Alexey Vikhlinin SCALING RELATIONS FOR LOW-MASS GALAXY CLUSTERS AND GROUPS
09800363 GO Andrew Fabian The X-ray Luminous Cluster underlying the Radio-Quiet Quasar H1821+643
09800379 GO Laurence David The Filamentary Structure of the Hot Gas in the NGC5044 Group
09800437 GO Roderick Johnstone The Link between optical nebulae and feedback in cluster cores
09800484 GO Lori Lubin The Active Galaxy Population in a Supercluster at z = 0.7
09800576 GO Sarah Gallagher Chandra/HST Coverage of Compact Galaxy Group Evolution
09800652 GO Aneta Siemiginowska The cluster around the powerful radio-loud quasar 3C186 at z=1.1
09800732 GO Graham Smith LoCuSS: Cluster Mass Comparison with Chandra and HST -- Observational Discrepancy or Agreement in the New Millennium?
09800842 GO JAN VRTILEK AWM 4: a sharp look at the core of a poor cluster stirred by AGN activity
09800847 LP Maxim Markevitch BOW SHOCK, ELECTRON-ION EQUILIBRIUM, BREAKUP OF COOL CORE, AND DARK SUBCLUSTER IN ABELL 520

Type: GTO/TOO

Proposal Number: 09800046

Title: Chandra Observations of SZ-selected Galaxy Clusters Detected by the South Pole Telescope

PI Name: Gordon Garmire

We propose a 200 ks program to for Chandra follow-up of some of the first massive galaxy clusters detected in the forthcoming South Pole Telescope (SPT) cluster survey. Our program (in conjunction with companion GTO observations by the HRC team) will provide a pathfinder for future much larger investments of Chandra time to follow-up the 200 most massive clusters detected in the SPT survey. This larger program will provide significant constraints on dark energy in its own right, and will greatly amplify the the cosmological power and reliability of the SPT survey.

R.A. Dec. Target Name Det. Grating Exp.Time
5:24:00.00 -54:30:00.00 SPT-6 ACIS-I NONE 20
5:24:00.00 -54:00:00.00 SPT-3 ACIS-I NONE 20
5:24:00.00 -53:30:00.00 SPT-9 ACIS-I NONE 20
5:30:00.00 -54:30:00.00 SPT-4 ACIS-I NONE 20
5:30:00.00 -54:00:00.00 SPT-1 ACIS-I NONE 20
5:30:00.00 -53:30:00.00 SPT-7 ACIS-I NONE 20
5:36:00.00 -54:30:00.00 SPT-5 ACIS-I NONE 20
5:36:00.00 -54:00:00.00 SPT-2 ACIS-I NONE 20
5:36:00.00 -53:30:00.00 SPT-8 ACIS-I NONE 20
23:30:00.00 -55:30:00.00 SPT-10 ACIS-I NONE 20

Type: GTO/TOO

Proposal Number: 09800120

Title: South Pole Telescope (SPT) - Chandra Cluster Cosmology

PI Name: Stephen Murray

We propose Chandra ACIS-I observations of a mass limited set of clusters detected by the South Pole Telescope using the redshift-independent Sunyaev-Zeldovich effect (SZE). This exploration will find the first clusters detected through their SZE signature on the cosmic microwave background. Ultimately, we expect to observe a sample of 200 clusters at z>0.5 with masses greater than 3x10^14 Msun. We will measure gas temperatures to an accuracy of better than 15% and gas masses to an accuracy of 8%. We will 1) combine the X-ray and SZE data to test d(z) 2) use the X-ray Y parameter (Y=M_gas * T_gas) to derive the cluster mass function which is a sensitive probe of cosmological parameters and 3) improve the reliability of cluster mass estimates using the X-ray mass proxies.

R.A. Dec. Target Name Det. Grating Exp.Time
0:00:00.00 0:00:00.00 SPT1 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT2 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT3 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT4 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT5 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT6 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT7 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT8 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT9 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT10 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT11 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT12 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT13 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT14 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT15 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT16 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT17 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT18 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT19 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT20 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT21 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT22 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT23 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT24 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT25 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT26 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT27 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT28 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT29 ACIS-I NONE 10
0:00:00.00 0:00:00.00 SPT30 ACIS-I NONE 10

Type: GO

Proposal Number: 09800154

Title: Characterisation of the most distant cluster of galaxies, JKCS041 at z=1.91

PI Name: Stefano Andreon

The number of high-redshift galaxy clusters is scarce, with only few systems known at z>1 and the highest cluster scoring z=1.45. We propose a 80 ks Chandra observation in order to characterise the most distant X-ray detected cluster of galaxies known thus far, JKCS041, at z=1.9, recently discovered by us and for which we have extensive imaging (radio, optical, near-infrared, mid-infrared, UV) data already in hand and spectroscopy in progress. These observations will ensure the first measure of X-ray properties of clusters at this distance and significantly enlarge the redshift baseline of the scaling relations.

R.A. Dec. Target Name Det. Grating Exp.Time
2:26:44.00 -4:41:45.00 JKCS 041 ACIS-S NONE 80

Type: LP

Proposal Number: 09800310

Title: Probing Dark Energy with Relaxed Galaxy Clusters

PI Name: Steven Allen

We seek to constrain dark energy using studies of the apparent evolution of the X-ray gas mass fraction in the most X-ray luminous, dynamically relaxed galaxy clusters. The proposed observations will improve the detection of the effects of dark energy from the X-ray data alone to > 5 sigma. More importantly, they will allow us to measure the level of intrinsic (systematic) scatter in distance measurements from this technique and establish whether this is smaller than from type Ia supernovae measurements. Used in combination with supernovae and CMB data, the new Chandra observations will allow the most precise search to date for evolution in the dark energy equation of state - our best approach in trying to understand the origin of cosmic acceleration.

R.A. Dec. Target Name Det. Grating Exp.Time
1:59:49.30 8:49:59.20 MACS0159 ACIS-I NONE 20
4:39:02.30 5:20:43.60 RXJ0439-0520 ACIS-I NONE 30
10:23:39.40 4:11:14.30 Zwicky 3146 ACIS-I NONE 40
11:15:52.10 1:29:52.90 MACS1115 ACIS-I NONE 40
13:11:01.60 -3:10:40.00 MACS1311 ACIS-I NONE 30
13:59:10.30 -19:29:24.40 MACS1359 ACIS-I NONE 50
14:27:16.20 44:07:31.00 MACS1427+44 ACIS-I NONE 40
14:27:39.40 -25:21:02.00 MACS1427-25 ACIS-I NONE 30
16:21:24.80 38:10:09.00 MACS1621 ACIS-I NONE 60
20:46:00.60 -34:30:17.00 MACS2046 ACIS-I NONE 40
21:29:39.90 0:05:20.00 RXJ2129+0005 ACIS-I NONE 30
22:29:45.30 -27:55:36.90 MACS2229 ACIS-I NONE 15
23:08:22.10 -2:11:29.10 Abell 2537 ACIS-I NONE 40

Type: GO

Proposal Number: 09800313

Title: Bubble heating in Extreme Cooling Clusters

PI Name: Steven Allen

Our proposal targets `extreme cooling' clusters: those systems with the largest, fastest cooling rates that most severely challenge the AGN-heating paradigm for cluster cores. By targeting two X-ray bright `extreme cooling cluters' with the clearest radio bubbles in their cores, we seek to establish whether it is possible for AGN heating to balance cooling in such systems. If cooling is not balanced by some heat source, then large residual cooling rates should be detectable in the spectral X-ray data. We will measure the bubble properties precisely and map the spatial-spectral structure of the surrounding X-ray gas, searching for ghost bubbles, shocks, ripples, fronts and non-thermal emission.

R.A. Dec. Target Name Det. Grating Exp.Time
19:31:49.60 -26:34:34.00 MACSJ1931.8-2634 ACIS-S NONE 100

Type: GO

Proposal Number: 09800349

Title: SCALING RELATIONS FOR LOW-MASS GALAXY CLUSTERS AND GROUPS

PI Name: Alexey Vikhlinin

Detailed measurements of the cluster scaling relations (e.g., L-T) require 1) large, objectively selected, statistically complete samples, and 2) observations that cover a large fraction of the system's virial radius. Such data are now available in the Chandra archive for a large number of high-M clusters, but not for the systems with T ~ 2 keV and below. We propose to fill this gap by observing a sample of 22 low-L objects from a new, sensitive X-ray survey. These observations will quadruple the statistics for low-T clusters and extend the reliable determination

R.A. Dec. Target Name Det. Grating Exp.Time
0:57:24.70 -26:16:49.00 cl0057-2616 ACIS-I NONE 10
2:37:59.60 -52:24:47.00 cl0237-5224 ACIS-I NONE 14
2:45:45.70 9:36:36.00 cl0245+0936 ACIS-I NONE 16
3:06:28.70 -9:43:50.00 cl0306-0943 ACIS-I NONE 10
3:27:54.50 2:33:47.00 cl0327+0233 ACIS-I NONE 11
3:34:03.30 -39:00:46.00 cl0334-3900 ACIS-I NONE 16
3:36:49.40 -28:04:53.00 cl0336-2804 ACIS-I NONE 11
3:40:27.20 -28:40:20.00 cl0340-2840 ACIS-I NONE 10
8:38:31.40 19:48:15.00 cl0838+1948 ACIS-I NONE 20
10:58:12.60 1:36:58.00 cl1058+0136 ACIS-I NONE 10
12:06:33.50 -7:44:24.00 cl1206-0744 ACIS-I NONE 10
12:59:51.00 31:20:48.00 cl1259+3120 ACIS-I NONE 18
13:49:00.20 49:18:33.00 cl1349+4918 ACIS-I NONE 19
15:33:17.10 31:08:55.00 cl1533+3108 ACIS-I NONE 10
16:30:14.70 24:34:47.00 cl1630+2434 ACIS-I NONE 10
22:20:09.10 -52:28:01.00 cl2220-5228 ACIS-I NONE 10

Type: GO

Proposal Number: 09800363

Title: The X-ray Luminous Cluster underlying the Radio-Quiet Quasar H1821+643

PI Name: Andrew Fabian

We propose to make a direct imaging study of the only low redshift galaxy cluster to contain a highly luminous quasar, H1821+643. Existing Chandra observations of the X-ray bright cluster are only noisy snapshots, having been performed using gratings, which much reduce the effective area, do not decrease the background, and produce diffraction spikes. Even these observations strongly hint at an interaction between the jets and outflows of the quasar on its surroundings, in terms of rings of brighter emission possibly indicating shocks. In addition the northern FRI lobe of the quasar also appears to be detected in emission. We expect to learn much about cluster-quasar interaction from this unique object.

R.A. Dec. Target Name Det. Grating Exp.Time
18:21:57.40 64:20:37.00 H1821+643 ACIS-S NONE 90

Type: GO

Proposal Number: 09800379

Title: The Filamentary Structure of the Hot Gas in the NGC5044 Group

PI Name: Laurence David

An early 20~ksec Chandra observation of the X-ray bright NGC 5044 group revealed an extensive system of cool X-ray filaments and cavities in the central region of the group. The similarity of these structures with those observed in other cooling flows suggests that they were produced AGN outbursts. We recently obtained GMRT data on NGC 5044 and detected 40 mJ of unresolved emission. NGC 5044 has also been extensively observed in the optical and IR (including a recent Spitzer observation). There is a strong spatial correlation between the $H_{\alpha}$ filaments, dust, and cool x-ray filaments in NGC 5044. We propose a 80~ksec Chandra observation of NGC5044 to determine the relationships between the radio emitting plasma, molecular gas, ionized gas, dust, and x-ray emitting gas.

R.A. Dec. Target Name Det. Grating Exp.Time
13:15:24.00 -16:23:06.80 NGC 5044 ACIS-S NONE 80

Type: GO

Proposal Number: 09800437

Title: The Link between optical nebulae and feedback in cluster cores

PI Name: Roderick Johnstone

The presence of luminous optical emission-line nebulae in brightest cluster galaxies is a dramatic marker for the presence of feedback or heating from the central active nucleus to the intracluster medium. Here we propose ACIS-S observations of the five brightest REFLEX clusters selected to have the most luminous optical emission-line nebulae. We shall confirm the link between emission-line gas and feedback and search for clues to the details of the heating mechanism by correlating the spatial distribution of feedback power with other cluster properties, for example, radio power or merger activity.

R.A. Dec. Target Name Det. Grating Exp.Time
10:23:50.80 -27:15:31.00 RXCJ1023.8-2715 ACIS-S NONE 40
14:59:29.30 -18:11:13.00 RXCJ1459.4-1811 ACIS-S NONE 40
15:24:12.80 -31:54:14.00 RXCJ1524.2-3154 ACIS-S NONE 40
15:58:23.20 -14:10:04.00 RXCJ1558.3-1410 ACIS-S NONE 40

Type: GO

Proposal Number: 09800484

Title: The Active Galaxy Population in a Supercluster at z = 0.7

PI Name: Lori Lubin

We propose to use Chandra and the VLA to map the active galaxy population in a supercluster at z = 0.7. The structure contains seven massive clusters and covers a 11 Mpc x 22 Mpc region. Combined with our extensive supporting data, the Chandra and VLA observations will allow us to measure the properties of X-ray and radio sources over a wide range of local densities, study AGN/starburst host galaxies to determine what causes gas-fueling events, and quantify the effect of large scale structure on the nuclear activity and gas content of galaxies. The proposed observations will be used to constrain how large-scale processes influence galaxy-scale events and are a natural continuation of our approved Cycle 7 & 8 programs to study superclusters and dynamically-active systems at high redshift.

R.A. Dec. Target Name Det. Grating Exp.Time
13:24:42.50 30:16:54.10 SC1324+3016 ACIS-I NONE 50
13:24:49.50 30:51:34.10 SC1324+3051 ACIS-I NONE 50

Type: GO

Proposal Number: 09800576

Title: Chandra/HST Coverage of Compact Galaxy Group Evolution

PI Name: Sarah Gallagher

The first galaxies and their environments differed substantially from those locally, with multiple interactions influencing their histories. Compared to all other nearby environments, present-day compact galaxy groups most closely reproduce conditions in the earlier universe (z~4) when galaxies assembled through hierarchical formation, and galaxy groups combined to form proto-clusters (in dense regions) or massive ellipticals (in the field). We propose senstitive Chandra observations of two nearby compact galaxy groups, HCGs 31 and 59, to complete a sample of six with joint Chandra/HST coverage. In addition to Spitzer mid-IR and Swift UV imaging already in hand, these data will enable a penetrating multiwavelength investigation into this important environment.

R.A. Dec. Target Name Det. Grating Exp.Time
5:01:38.00 -4:15:25.00 HCG 31 ACIS-S NONE 39
11:48:27.00 12:42:40.00 HCG 59 ACIS-S NONE 39

Type: GO

Proposal Number: 09800652

Title: The cluster around the powerful radio-loud quasar 3C186 at z=1.1

PI Name: Aneta Siemiginowska

We request a 200~ksec deep Chandra ACIS-S observation of the high redshift, z=1.1 X-ray cluster associated with the radio-loud quasar 3C~186. We will detect the X-ray cluster emission up to ~0.5~Mpc away from the quasar, study its morphology, and look for an excess temperature as a signature of interaction or a merging process in this high redshift cluster. This cluster is associated with a powerful young quasar (L_bol ~ 10^47 erg/sec) and it gives us a rare opportunity to study an early phase of the interaction between a quasar and its surrounding intracluster medium.

R.A. Dec. Target Name Det. Grating Exp.Time
7:44:17.40 37:53:17.10 3C 186 ACIS-S NONE 40
7:44:17.40 37:53:17.10 3C 186 ACIS-S NONE 160

Type: GO

Proposal Number: 09800732

Title: LoCuSS: Cluster Mass Comparison with Chandra and HST -- Observational Discrepancy or Agreement in the New Millennium?

PI Name: Graham Smith

We propose ACIS-I observations of 15 (Lx>1E44erg/s) galaxy clusters at z=0.2 that we have recently imaged with HST. With existing data on 11 clusters, these new data will form a unique high quality Chandra/HST dataset because the sample of 26 is completely unbiased with respect to their X-ray properties. Within the Local Cluster Substructure Survey (LoCuSS) we propose to use these data to characterise the systematic uncertainties in X-ray and lensing mass measurements within cluster cores - essential ground-work for cluster cosmology experiments which rely on precise cluster mass measurements. We will use mock cluster observations based on the Millennium Simulations to calibrate our observational measurements and new constraints on cluster physics to further improve the simulations.

R.A. Dec. Target Name Det. Grating Exp.Time
0:43:23.10 -20:37:35.00 RXCJ0043.4-2037 ACIS-I NONE 20
1:05:37.20 -24:35:57.00 RXCJ0105.5-2439 ACIS-I NONE 20
1:18:04.50 -27:00:13.00 RXCJ0118.1-2658 ACIS-I NONE 20
2:20:56.80 -38:29:02.00 RXCJ0220.9-3829 ACIS-I NONE 20
2:37:24.60 -26:30:02.00 RXCJ0237.4-2630 ACIS-I NONE 20
3:04:03.60 -36:57:21.00 RXCJ0304.1-3656 ACIS-I NONE 20
3:07:01.10 -28:40:30.00 RXCJ0307.0-2840 ACIS-I NONE 20
3:31:07.60 -21:00:15.00 RXCJ0331.1-2100 ACIS-I NONE 20
3:36:17.30 -40:38:09.00 RXCJ0336.3-4037 ACIS-I NONE 20
4:49:54.70 -44:40:55.00 RXCJ0449.9-4440 ACIS-I NONE 20
5:28:15.40 -29:42:57.00 RXCJ0528.2-2942 ACIS-I NONE 20
5:47:34.20 -31:53:01.00 RXCJ0547.6-3152 ACIS-I NONE 20
6:38:51.20 -53:57:47.00 RXCJ0638.7-5358 ACIS-I NONE 20
10:00:28.90 44:09:10.00 RXCJ1000.5+4409 ACIS-I NONE 20
16:24:16.20 41:15:10.00 Abell 2187 ACIS-I NONE 20

Type: GO

Proposal Number: 09800842

Title: AWM 4: a sharp look at the core of a poor cluster stirred by AGN activity

PI Name: JAN VRTILEK

The central regions of galaxy clusters, frequently occupied by massive elliptical galaxies with strong radio sources interacting with dense, X-ray emitting gas, are among the most interesting and physically active regions in the Universe. We here propose a deep observation of AWM 4, a poor cluster of relaxed appearance without a cooling core but with strong evidence of AGN-driven heating and gas mixing. In this unusual object we will examine the interaction between cluster gas and radio source at high resolution, measure the properties of the gas and constrain the energy budget of the radio source, and clarify the nature of the observed abundance irregularities.

R.A. Dec. Target Name Det. Grating Exp.Time
16:04:56.80 23:55:56.00 AWM 4 ACIS-S NONE 80

Type: LP

Proposal Number: 09800847

Title: BOW SHOCK, ELECTRON-ION EQUILIBRIUM, BREAKUP OF COOL CORE, AND DARK SUBCLUSTER IN ABELL 520

PI Name: Maxim Markevitch

Shock fronts provide a unique tool to study the cluster plasma. Only two have been found, those in 1E0657 and A520. Using a long observation of 1E0657, we have determined, for the first time in any astrophysical plasma, that electron-proton equilibration time is shorter than Coulomb - a tantalizing result but based on one object. A520 gives the only chance to confirm it. Its shock also coincides with an edge of the radio halo, enabling tests of the origin of the intracluster relativistic electrons. A520 also exhibits a remnant of a cool core broken up by merger-induced instabilities, providing data on plasma viscosity. Finally, weak lensing map of A520 reveals an intriguing dark subcluster almost devoid of galaxies. We propose a long observation of this exceptionally interesting cluster.

R.A. Dec. Target Name Det. Grating Exp.Time
4:54:05.40 2:53:35.00 A520_OFF1 ACIS-I NONE 115
4:54:05.40 2:53:35.00 A520_OFF2 ACIS-I NONE 115
4:54:05.40 2:53:35.00 A520_OFF3 ACIS-I NONE 115
4:54:05.40 2:53:35.00 A520_OFF4 ACIS-I NONE 115

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